Science

I see in the NYT that there’s a new “authorized biography” of the Bangles, recounting their rise and fall. An excerpt:

The first time Susanna Hoffs and the Peterson sisters sang together and their voices blended, the frisson was unmistakable. “We knew we had something,” Hoffs said. “We created a band in that moment.”

Hoffs, 66, beamed at the memory, sitting in her kitchen on a late January afternoon. Dressed in a sweater and slacks, the diminutive [she’s 5″2′] singer and guitarist sipped coffee, an old Margaret Keane painting hanging above her. Her airy home in Brentwood is just a few blocks from where the Bangles were born, on a cool evening in early 1981 in her parents’ garage.

“It’s an overused word, but we were organic,” the guitarist Vicki Peterson, 67, said. “We formed ourselves, played the music we loved, we really were a garage band.” But a garage band “that somehow became pop stars,” the drummer Debbi Peterson, 63, noted. Both sisters were interviewed in video conversations.

The Bangles broke big, scoring five Top 5 hits and storming MTV with inescapable songs like “Manic Monday” and “Eternal Flame.” They were one of the era’s rare all-girl groups — and became one of the most successful female bands of all time — a crew of puckish 20-somethings showcasing their collective songwriting and vocal chops.

But one of the defining bands of the 1980s also ended in spectacular fashion. Less than a decade after its birth, the group imploded in its manager’s Hollywood mansion, the sisterhood of its members lost amid a farrago of fame and mental fatigue.

That story plays out vividly in “Eternal Flame: The Authorized Biography of the Bangles” by Jennifer Otter Bickerdike, out on Feb. 18. Bickerdike — the author of books about Nico and Britney Spears — fashioned a history of a bygone era in the music business, one in which the outsize influence of major labels, domineering producers and Machiavellian managers could routinely make or break a band.

. . . The notion of the Bangles as a band of equals quickly went out the window. “Susanna [Hoffs] was pushed forward as the sex symbol,” Bickerdike said. “But Sue is really smart and goofy, she’s actually kind of a dork, you know? So I think that was an uncomfortable role for her.”

And this is a crime:

While the Go-Go’s were inducted into the Rock & Roll Hall of Fame in 2021, the Bangles have yet to be nominated.

Here’s Susannah singing my favorite Bangles song, “Eternal Flame,” for which she wrote the lyrics, in 2021—when she was sixty (she turned 66 on January 17). She remains beautiful and alluring, and her voice is still lovely. She’s also Jewish, and I’d marry her in a second—if she wasn’t already married.

Here’s a good live version (1996) with just Hoffs and a guitarist. A live version with all the Bangles is here and you can hear the original recording here.  The song topped the charts in both the U.S. and U.K.

A comprehensive analysis pours cold water on claims that using carbon dioxide captured from the atmosphere to drive oil extraction can result in carbon-neutral fossil fuel

Software developers entering the International Obfuscated C Code Contest must write programs that look baffling, but perform unusual, unexpected or catastrophic tasks

Researchers are designing a global real-time monitoring system to help save the world's coral reefs from further decline, primarily due to bleaching caused by global warming.

When massive stars reach the end of their life cycle, they undergo gravitational collapse and shed their outer layers in a massive explosion (a supernova). Whereas particularly massive stars will leave a black hole in their wake, others leave behind a stellar remnant known as a neutron star (or white dwarf). These objects concentrate a mass greater than the entire Solar System into a volume measuring (on average) just 20 km (~12.5 mi) in diameter. Meanwhile, the extreme conditions inside neutron stars are still a mystery to astronomers.

In 2017, the first collision between two neutron stars was detected from the gravitational waves (GWs) it produced. Since then, astronomers have theorized how GWs could be used to probe the interiors of neutron stars and learn more about the extreme physics taking place. According to new research by a team from Goethe University Frankfurt and other institutions, the GWs produced by binary neutron star (BNS) mergers mere milliseconds after they merge could be the best means of probing the interiors of these mysterious objects.

The research was conducted by a group led by Luciano Rezzolla, a professor from the Institute for Theoretical Physics (ITP) at Goethe University and a Senior Fellow with the Frankfurt Institute for Advanced Studies (FIAS). The research team also includes members of the ExtreMe Matter Institute (EMMI-GSI), Darmstadt Technical University (TU Darmstadt), and the University of Stavanger in Norway. The paper detailing their findings appeared on February 3rd in Nature Communications.

Light bursts from the collision of two neutron stars. Credit: NASA’s Goddard Space Flight Center/CI Lab

Originally predicted by Einstein’s Theory of General Relativity (GR), gravitational waves are ripples in spacetime caused by the merger of massive objects (like white dwarfs and black holes). While the most intense GWs are produced from mergers, BNS emit GWs for millions of years as they spiral inward toward each other. The post-merger remnant (a massive, rapidly rotating object) also emits GWs in a strong but narrow frequency range. This last signal, the team argues, could hold crucial information about how nuclear matter behaves at extreme densities and pressures (aka. “equation of state“).

As the team explained in their paper, the amplitude of post-merger GWs behaves like a tuning fork after it is struck. This means that the GW signal goes through a phase (which they have named the “long ringdown”) where it increasingly trends toward a single frequency. Using advanced simulations of merging neutron stars, the team identified a strong connection between these unique characteristics and the properties of the densest regions in the core of neutron stars. As Dr. Rezzolla explained in a University of Goethe press release:

“Thanks to advances in statistical modeling and high-precision simulations on Germany’s most powerful supercomputers, we have discovered a new phase of the long ringdown in neutron star mergers. It has the potential to provide new and stringent constraints on the state of matter in neutron stars. This finding paves the way for a better understanding of dense neutron star matter, especially as new events are observed in the future.”

By analyzing the long ringdown phase, they argue, astronomers can significantly reduce uncertainties in the equation of state for neutron stars. “By cleverly selecting a few equations of state, we were able to effectively simulate the results of a full statistical ensemble of matter models with considerably less effort,” said co-author Dr. Tyler Gorda. “Not only does this result in less computer time and energy consumption, but it also gives us confidence that our results are robust and will be applicable to whatever equation of state actually occurs in nature.“

An artist’s concept of how LISA will work to detect gravitational waves from orbit in space. Credit: ESA

In this sense, post-merger neutron stars could be used as “tuning forks” for investigating some of the deepest cosmic mysteries. Said Dr. Christian Ecker, an ITP postdoctoral student, and the study’s lead author:

“Just like tuning forks of different material will have different pure tones, remnants described by different equations of state will ring down at different frequencies. The detection of this signal thus has the potential to reveal what neutron stars are made of. I am particularly proud of this work as it constitutes exemplary evidence of the excellence of Frankfurt- and Darmstadt-based scientists in the study of neutron stars.”

This research, added Dr. Ecker, compliments the work of the Exploring the Universe from Microscopic to Macroscopic Scales (ELEMENTS) research cluster. Located at the Giersch Science Center (GSC), this cluster combines the resources of Goethe University, TU Darmstadt, Justus Liebig University Giessen (JLU-Gießen), and the Facility for Antiproton and Ion Research (GSI-FAIR). Their aim is to combine the study of elementary particles and large astrophysical objects with the ultimate goal of finding the origins of heavy metals (i.e. platinum, gold, etc.) in the Universe.

While existing GW observatories have not detected post-merger signals, scientists are optimistic that next-generation instruments will. This includes the Einstein Telescope (ET), a proposed underground observatory expected to become operational in the next decade, and the ESA’s Laser Interferometer Space Antenna (LISA), the first GW observatory ever proposed for space, currently scheduled for deployment by 2035. With the completion of these and other third-generation GW observatories, the long ringdown could serve as a powerful means for probing the laws of physics under the most extreme conditions.

Further Reading: Goethe University

The post To Probe the Interior of Neutron Stars, We Must Study the Gravitational Waves from their Collisions appeared first on Universe Today.

Planets are born in swirling disks of gas and dust around young stars. Astronomers are keenly interested in the planet formation process, and understanding that process is one of the JWST’s main science goals. PDS 70 is a nearby star with two nascent planets forming in its disk, two of the very few exoplanets that astronomers have directly imaged.

Researchers developed a new, innovative approach to observing PDS 70 with the JWST and uncovered more details about the system, including the possible presence of a third planet.

PDS 70 is an orange dwarf star about 370 light-years away and hosts two young, growing planets: PDS 70b and PDS 70c. The European Southern Observatory’s Very Large Telescope (VLT) imaged both of the planets directly, and PDS 70b has the distinction of being the very first protoplanet every imaged directly. The VLT accomplished the feat in 2018 with its groundbreaking SPHERE instrument.

The SPHERE observations, along with other observations, allowed astronomers to get a much more detailed look at the planets’ atmospheres, masses, and temperatures.

Now, the JWST has taken another look at the pair of young planets. The results are in a new paper in The Astronomical Journal. It’s titled “The James Webb Interferometer: Space-based Interferometric Detections of PDS 70 b and c at 4.8 ?m,” and the lead author is Dori Blakely. Blakely is a grad student in Physics and Astronomy at the University of Victoria, BC, Canada.

The JWST’s Near Infrared Imager and Slitless Spectrograph (NIRISS) has a feature called Aperture Masking Interferometry (AMI), which allows it to function as an interferometer. It uses a special mask with tiny holes over the telescope’s primary mirror. The interferogram it creates has a much higher resolution because the effective size of the telescope becomes much larger.

“In this work, we present James Webb Interferometer observations of PDS 70 with the NIRISS F480M filter, the first space-based interferometric observations of this system,” the authors write. They found evidence of material surrounding PDS 70 b and c, which strengthens the idea that the planets are still forming.

“This is like seeing a family photo of our solar system when it was just a toddler. It’s incredible to think about how much we can learn from one system,” lead author Blakely said in a press release.

This is a colour-enhanced image of millimetre-wave radio signals from the ALMA observatory from previous research. It shows the PDS 70 star and both exoplanets. Image Credit: A. Isella, ALMA (ESO/NAOJ/NRAO)

Previous observations of the PDS 70 planets were made at shorter wavelengths, which were best explained by models for low-mass stars and brown dwarfs. But the JWST observed them at longer wavelengths, the longest they’d ever been observed with. These observations detected more light than previous observations, and the low-mass/brown dwarf models couldn’t account for the light.

The JWST observations hint at the presence of warm material around both planets, which is interpreted as material accreting from a circumplanetary disk. “Our photometry of both PDS 70 b and c provides tentative evidence of mid-IR circumplanetary disk emission through fitting spectral energy distribution models to these new measurements and those found in the literature,” the authors write.

This image from the study shows PDS 70 and its two planets with circumplanetary disks. The disks indicate that the planets are still growing by accumulating material, likely gas, from their disks. The larger orange feature is part of the larger disk surrounding the star and the planets. Image Credit: Blakely et al. 2025.

The results indicate that PDS 70 and its planets are vying for the same material needed to grow larger. The star is a T-Tauri star that’s only about 5.4 million years old. It won’t reach the Main Sequence for tens of millions more years and is still actively accreting material.

“These observations give us an incredible opportunity to witness planet formation as it happens,” said co-author Doug Johnstone from the Herzberg Astronomy and Astrophysics Research Centre. “Seeing planets in the act of accreting material helps us answer long-standing questions about how planetary systems form and evolve. It’s like watching a solar system being built before our very eyes.”

The new research also presents additional evidence supporting a third planet around the stars, putatively named PDS 70d.

A 2024 paper presented hints of a third planet. However, there was much uncertainty. The authors of that paper wrote that they may have found another exoplanet, but it could also be a dust clump or an inner spiral of material. “Follow-up studies of d are therefore especially exciting,” the authors wrote.

While this new research isn’t solely a follow-up study on the potential exoplanet, it has constrained some of the object’s properties, whatever it may be.

This image from the research shows PDS 70 and the two planets. On the right side of the image is part of the larger circumstellar disk. This image shows increased emissions as a bright triangle. Current observations can’t discern whether this is a disk feature, a spiral or clumpy structure of gas, a stream of gas between PDS 70 b and c, or an additional planet, as suggested by previous research. Image Credit: Blakely et al. 2024.

If there is a third planet, it is significantly different from the other two. “… if the previously observed emission at shorter wavelengths is due to a planet, this putative planet has a different atmospheric composition than PDS 70 b or c,” the authors explain.

“Follow-up observations will be needed to determine the nature of this emission.”

The post The JWST Gives Us Our Best Image of Planets Forming Around a Star appeared first on Universe Today.

A biohybrid hand which can move objects and do a scissor gesture has been created. The researchers used thin strings of lab-grown muscle tissue bundled into sushilike rolls to give the fingers enough strength to contract. These multiple muscle tissue actuators (MuMuTAs), created by the researchers, are a major development towards building larger biohybrid limbs. While currently limited to the lab environment, MuMuTAs have the potential to advance future biohybrid prosthetics, aid drug testing on muscle tissue and broaden the potential of biohybrid robotics to mimic real-life forms.

A biohybrid hand which can move objects and do a scissor gesture has been created. The researchers used thin strings of lab-grown muscle tissue bundled into sushilike rolls to give the fingers enough strength to contract. These multiple muscle tissue actuators (MuMuTAs), created by the researchers, are a major development towards building larger biohybrid limbs. While currently limited to the lab environment, MuMuTAs have the potential to advance future biohybrid prosthetics, aid drug testing on muscle tissue and broaden the potential of biohybrid robotics to mimic real-life forms.

Researchers have achieved a breakthrough in wearable health technology by developing a novel self-healing electronic skin (E-Skin) that repairs itself in seconds after damage. This could potentially transform the landscape of personal health monitoring.

Researchers have achieved a breakthrough in wearable health technology by developing a novel self-healing electronic skin (E-Skin) that repairs itself in seconds after damage. This could potentially transform the landscape of personal health monitoring.

Children may have a higher risk of developing ADHD if their mothers used paracetamol – also known as acetaminophen – during pregnancy, adding weight to the contested link between the painkiller and fetal brain development

Sometimes, things across the vast Universe line up just right for us. The Einstein Ring above, like all Einstein Rings, has three parts. In the foreground is a distant massive object like a galaxy or galaxy cluster. In the background, at an even greater distance away, is a star or another galaxy.

We’re the observers, the third part, and all three must be perfectly aligned for an Einstein Ring to appear.

An Einstein Ring (ER) works by gravitational lensing. The massive foreground object has such powerful gravity that it bends space-time, which means the light from the distant object follows a curved path. The light is magnified and shaped into a circle.

Einstein Rings are intriguing visual oddities, but they’re also powerful, naturally occurring scientific tools.

“All strong lenses are special, because they’re so rare, and they’re incredibly useful scientifically.”

Conor O’Riordan, Max Planck Institute for Astrophysics, Germany A close-up view of the centre of the NGC 6505 galaxy, with the bright Einstein ring around its nucleus, captured by ESA’s Euclid space telescope. Image Credit: ESA/Euclid/Euclid Consortium/NASA, image processing by J.-C. Cuillandre, G. Anselmi, T. Li. LICENCE CC BY-SA 3.0 IGO or ESA Standard Licence

In this ER, the massive foreground object is the galaxy NGC 6505, which is warping spacetime around it. The galaxy is not unique—it just happens to be massive and about 600 million light-years away.

The background galaxy is also not particularly special. It’s 4.42 billion light years away, has never been seen before, and doesn’t even have a name. We’re only seeing it because of the alignment between both galaxies and us.

The ESA launched Euclid in July 2023, and its job is to measure the redshift of galaxies. In doing so, it can measure the expansion of the Universe so we can hopefully make progress in understanding dark energy and dark matter.

After launch, Euclid went through a testing phase and sent images back to us. For testing reasons, they were deliberately out of focus. Bruno Altieri, a scientist on the Euclid team, thought he saw something unusual in one of the images.

“I look at the data from Euclid as it comes in,” Bruno explained in a press release. “Even from that first observation, I could see it, but after Euclid made more observations of the area, we could see a perfect Einstein ring. For me, with a lifelong interest in gravitational lensing, that was amazing.”

Astronomers have observed NGC 6505, the foreground galaxy, many times, but they’ve never seen the ring before. After Altieri spotted the ring, Euclid’s high-resolution instruments captured follow-up images of it with the ring in focus. The instruments are VIS, the Visible light camera, and NISP, the Near-Infrared Spectrometer and Photometer.

“This demonstrates how powerful Euclid is, finding new things even in places we thought we knew well.”

Valeria Pettorino, ESA Euclid Project Scientist.

“I find it very intriguing that this ring was observed within a well-known galaxy, which was first discovered in 1884,” says Valeria Pettorino, ESA Euclid Project Scientist. “The galaxy has been known to astronomers for a very long time. And yet, this ring was never observed before. This demonstrates how powerful Euclid is, finding new things even in places we thought we knew well. This discovery is very encouraging for the future of the Euclid mission and demonstrates its fantastic capabilities.”

Research based on Euclid’s findings was published in the journal Astronomy and Astrophysics. It’s titled “Euclid: A complete Einstein ring in NGC 6505.” The lead author is Conor O’Riordan of the Max Planck Institute for Astrophysics in Germany.

“An Einstein ring is an example of strong gravitational lensing,” explained O’Riordan. “All strong lenses are special, because they’re so rare, and they’re incredibly useful scientifically. This one is particularly special, because it’s so close to Earth and the alignment makes it very beautiful.”

“The combination of the low redshift of the lens galaxy, the brightness of the source galaxy, and the completeness of the ring make this an exceptionally rare strong lens, unidentified until its observation by Euclid,” the authors write in their paper. The researchers used Euclid’s instruments and the Keck Cosmic Web Imager (KCWI) to observe the ring. “The Euclid imaging, in particular, presents one of the highest signal-to-noise ratio optical/near-infrared observations of a strong gravitational lens to date.”

Strong lenses like this one allow astronomers to study the background galaxy, which would otherwise be impossible. These lenses also hold information about the expansion of the Universe, dark energy, and dark matter. “Strong lenses can be used as ‘cosmic telescopes’ to achieve higher spatial resolution when studying the lensed sources, and to test general relativity,” the authors explain in their research.

The authors also point out that studying the lens itself is also beneficial. “The most prevalent application of galaxy-scale strong lensing is in studying the lens itself, which is most often an early-type galaxy (ETG),” they write. All elliptical galaxies are considered early-type galaxies.

This image shows Euclid imaging data used in this work and in which Altieri’s lens was discovered. The main panel shows a composite false-colour image produced by combining the VIS and NISP data. The inset shows only the higher-resolution VIS data in the central 8? of the image, indicated by the square in the main panel. Image Credit: O’Riordan et al. 2025.

“Low redshift lenses are intrinsically rare because there is very little volume at low redshift,” the researchers explain in their paper. “That we observed one in the early days of Euclid is unremarkable, but for it to be an obvious strong lens is quite exceptional.”

Euclid’s mission is scheduled to last six years. The researchers say that while the spacecraft will find more Einstein rings during its mission, as many as 100,000, it will likely never find another one like this. “The exceptional nature of Altieri’s lens means it is unlikely that Euclid will find another lens below z?=?0.05 with a ring as bright as that observed here,” they explain.

The lens’ low redshift makes it exceptionally valuable scientifically. Only five others have similar low redshifts. “Strong lenses at low redshift have Einstein radii that are comparatively small in physical terms and allow for a detailed study of the composition and structure of the central region of the galaxy,” the authors write.

The researchers were able to determine the lens galaxy’s peculiar velocity, an important step in understanding Universal expansion, dark matter, and dark energy. They were also able to model its light profile in detail.

The paper is open access and interested readers can find more info there.

Press Release: Euclid discovers a stunning Einstein ring

Published Research: Euclid: A complete Einstein ring in NGC 6505

The post The Euclid Space Telescope Captures a Rare, Stunning Einstein Ring appeared first on Universe Today.

A new study has revealed the clearest-ever picture of the surface chemistry of worm species that provides groundbreaking insights into how animals interact with their environment and each other. These discoveries could pave the way for strategies to deepen our understanding of evolutionary adaptations, refine behavioural research, and ultimately overcome parasitic infections.

Scientists have demonstrated that negative refraction can be achieved using atomic arrays -- without the need for artificially manufactured metamaterials. Scientists have long sought to control light in ways that appear to defy the laws of Nature. Negative refraction -- a phenomenon where light bends in the opposite direction to its usual behavior -- has captivated researchers for its potential to revolutionize optics, enabling transformative technologies such as superlenses and cloaking devices. Now, carefully arranged arrays of atoms have brought these possibilities a step closer, achieving negative refraction without the need for artificially manufactured metamaterials.

Using genes borrowed from bacteria, researchers have demonstrated fish and flies can be engineered to break down methylmercury and remove it from their bodies as a less harmful gas, offering new ways to tackle one of the world's most dangerous pollutants.

Scientists have used holographic projections to bring unprecedented resolution to a light-based 3D printing technique. The method allows the fabrication of millimeter-scale objects within seconds using significantly less energy than previous approaches.

Scientists have used holographic projections to bring unprecedented resolution to a light-based 3D printing technique. The method allows the fabrication of millimeter-scale objects within seconds using significantly less energy than previous approaches.

Our Sun is a giant plasma windbag spewing a constant stream of charged particles called the solar wind. This stream leaves the Sun at speeds around 400 to 800 kilometers per second and extends to the outer edge of the Solar System to about 125 astronomical units. Astronomers have long wondered about what feeds this powerful outflow.

Recently the ESA Solar Orbiter spacecraft observed tiny plasma jets a few hundred kilometers wide, occurring across the Sun. Each one flashes for a brief instant above the solar surface. Just as a tiny stream expands to create a raging river here on Earth, these minuscule jets combine to provide “background” power that blossoms into the fast and slow parts of the solar wind.

Probing the Solar Wind

A research team led by Lakshmi Pradeep Chitta at the Max Planck Institute for Solar System Research, Germany used the probe’s onboard ‘cameras’ to spot more tiny jets within coronal holes close to the Sun’s equator. “We could only detect these tiny jets because of the unprecedented high-resolution, high-cadence images produced by EUI,” said Chitta at the time of their discovery in 2023. They used the extreme ultraviolet channel of EUI’s high-resolution imager, which observes million-degree solar plasma at a wavelength of 17.4 nanometers. At the time, scientists suspected these flares were at the heart of solar wind generation but didn’t understand how widespread they were.

The team continued to use the Polarimetric and Helioseismic Imager (PHI), Solar Wind Plasma Analyser (SWA) and Magnetometer (MAG) to study the jets over the past year and a half. By combining these high-resolution images with direct measurements of the stream of particles and the Sun’s magnetic field around the Solar Orbiter, the researchers spotted more tiny flares within coronal holes close to the solar equator. Based on those observations, they directly connected the solar wind measured at the spacecraft back to those same jets.

Picoflares that power the solar wind occur across the solar surface. Courtesy ESA. The Solar Wind and its Effects

For many years, the solar wind has remained something of a challenge to understand. We can certainly see its effects in the form of variable space weather. During years of solar maximum, the Sun is more active. That powers more outbursts in the form of X-class flares and coronal mass ejections that extend out for millions of kilometers. When the Sun quiets down, so does the activity, although it never completely stops.

On Earth, we see the effects of the solar wind in increased auroral displays, and—if coronal mass ejections are severe—in disruption of communication and power generation technologies. Out in space, the solar wind also affects other solar system bodies. For example, it shapes and disrupts comet plasma tails as they near their closest approach to the Sun. But, what powers it? And, how do scientists explain its variations?

The solar wind comes in two flavors: slow and dense at the solar equatorial regions and fast and not-so-dense at the higher latitudes and the poles. The Ulysses spacecraft, which was in a near-polar orbit for nearly 18 years starting in 1990, mapped these regions of the solar wind closest to the Sun and found that the fast wind is relatively steady, while the slow solar wind is more variable in speed.

The fast solar wind comes from the direction of dark patches in the Sun’s atmosphere called coronal holes. These are places where the solar magnetic field stretches out from the Sun through the solar system. Charged particles can flow along these “open” magnetic field lines, heading away from the Sun as the solar wind. It turns out that the slow solar wind also comes from equatorial coronal holes where nanoflares are also at work.

More about the Jets

So, what causes these tiny jets? Such nanoflare outbursts are called “picoflare jets”. They’re powered by a process called “magnetic reconnection.” This happens when magnetic field lines in a region of the Sun’s atmosphere get tangled and twisted together. Eventually, they break, similar to what happens when you twist a rubber band too much. That “break” releases heat and energy into the corona. New field lines reconnect to continue the process. This is the same mechanism that powers larger solar flares.

Interestingly, we see similar magnetic reconnection in comet plasma tails. Magnetic field lines are entrained in the solar wind. They “drape” around a comet and its plasma tail. Those field lines have a specific polarity. As the comet passes through different “regimes” of the solar wind, it experiences different polarities. When that happens, the old-polarity plasma tail “breaks off” in a disconnection event and that releases energy. The new field lines build a new plasma tail in a case of magnetic reconnection.

Comets are small-scale examples of this effect, while the Sun is a perfect example of the large-scale influence of magnetic reconnection. When you have countless numbers of these nanoflares releasing energy into the corona, it’s enough to power the entire solar wind. Spacecraft such as the Solar Orbiter and the Parker Solar Probe have front-row seats to the action and will provide long-term measurements of the Sun’s tremendous power-generation action.

For More Information

Scientists Spot Tiny Sun Jets Driving Fast and Slow Solar Wind
Coronal Hole Picflare Jets are Progenitors of Both Fast and Alfvénic Slow Solar Wind
Solar Wind

The post Tiny Solar Jets Drive the Sun’s Fast and Slow Solar Wind appeared first on Universe Today.

A team of researchers succeeded in adapting an AI system to reliably assist with making nanoparticle measurements which speeds up the research process significantly.

A team of researchers succeeded in adapting an AI system to reliably assist with making nanoparticle measurements which speeds up the research process significantly.